Possibility of unique detection of primordial black hole gamma-ray bursts

Cline, D.; Hong, Woo-Pyo

doi:10.1086/186670

Cited by 43 publications

(34 citation statements)

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“…Similar comments apply to attempts to link PBHs with specific observational phenomena. It has been suggested, for instance, that PBHs with the right mass could be responsible for certain classes of γ-ray bursts [413,414,415], or for long-term quasar variability via microlensing [416,417]. Other possible connections have been drawn to diffuse γ-ray emission from the Galactic halo [418,419] and the Macho microlensing events [420,421].…”

Section: Primordial Black Holesmentioning

confidence: 99%

Dark matter and background light

2004

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Section: Primordial Black Holesmentioning

confidence: 99%

Dark matter and background light

2004

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“…Rare interactions could slightly modify the γ, p,p, e + , e − , ν and ν signatures of PBHs but not significantly. Other authors, such Belyanin, Kocharovsky, and Kocharovsky [22] and D. Cline et al [6,8], have proposed photosphere models which are unrelated to the Heckler mechanism. These models are mainly motivated by an attempt to explain certain short-period gamma-ray bursts.…”

Section: Introductionmentioning

confidence: 99%

“…[5]). To date, no such PBH burst or background has been conclusively detected, although D. Cline et al [6,7,8] have attributed some short-timescale gamma-ray bursts to PBH explosions. However, observations of the 100 MeV gamma-ray background imply that 10 15 g PBHs must have Ω pbh 10 −8 [4], where Ω pbh is their present density in units of the critical density.…”

Section: Introductionmentioning

confidence: 99%

Do evaporating black holes form photospheres?

2008

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Several authors, most notably Heckler, have claimed that the observable Hawking emission from a microscopic black hole is significantly modified by the formation of a photosphere around the black hole due to QED or QCD interactions between the emitted particles. In this paper we analyze these claims and identify a number of physical and geometrical effects which invalidate these scenarios. We point out two key problems. First, the interacting particles must be causally connected to interact, and this condition is satisfied by only a small fraction of the emitted particles close to the black hole. Second, a scattered particle requires a distance ∼ E/m 2 e for completing each bremsstrahlung interaction, with the consequence that it is improbable for there to be more than one complete bremsstrahlung interaction per particle near the black hole. These two effects have not been included in previous analyses. We conclude that the emitted particles do not interact sufficiently to form a QED photosphere. Similar arguments apply in the QCD case and prevent a QCD photosphere (chromosphere) developing when the black hole temperature is much greater than ΛQCD, the threshold for QCD particle emission. Additional QCD phenomenological arguments rule out the development of a chromosphere around black hole temperatures of order ΛQCD. In all cases, the observational signatures of a cosmic or Galactic halo background of primordial black holes or an individual black hole remain essentially those of the standard Hawking model, with little change to the detection probability. We also consider the possibility, as proposed by Belyanin et al. and D. Cline et al., that plasma interactions between the emitted particles form a photosphere, and we conclude that this scenario too is not supported.

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“…According to [107], PBHs with masses less than about 5 × 10 11 kg would have evaporated by now. These evaporating PBHs can be detected through their Hawking radiation, and may appear as very short bursts as modeled in [110], with time durations of the order of 0.1 s and with a luminosity of about 10 33 erg/s. From what has been stated s no asonable to conclude that black holes are intimately involved in the production of all three classes of GRBs: long, short, and very short bursts.…”

Section: )mentioning

confidence: 99%

Supermassive Black Holes, the Early Universe, and Gamma-Ray Bursts

Dallal¹,

Azzam²

2013

JMP

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Observational evidence reveals that supermassive black holes reside at the center of most galaxies up to the furthest observable redshifts. The tight M-σ relation suggests a close operative feedback between the growth of supermassive black holes and the growth of the galactic bulge. Models describing the formation scenarios of seeding black holes and their growth are reviewed. In each of these models, the prevailing environments in the primordial-galactic disks, including the gas dynamics, cooling processes, and metallic enrichment are explored. It is shown that the galactic disk parameters set constraints on the channel of formation of the seeding black holes and their growth. Primordial black holes from the inflationary era, their formation, possible interaction, and constraints on their observations are discussed. Gamma-ray bursts resulting either from the collapse of massive stars, or from the collision of compact objects are explored. The abundance of these violent events in the early universe suggests a possible connection with galaxy formation.

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Possibility of unique detection of primordial black hole gamma-ray bursts

Cited by 43 publications

References 0 publications

Dark matter and background light

Dark matter and background light

Do evaporating black holes form photospheres?

Supermassive Black Holes, the Early Universe, and Gamma-Ray Bursts

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